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3D Spectroscopy of Blue Compact Galaxies. Diagnostic Diagrams

Ismael Martınez-Delgado1 , Guillermo Tenorio-Tagle2, Casiana Munoz-Tunon1, Alexei V.

Moiseev3

and

Luz M. Cairos4

Instituto de Astrofısica de Canarias, Vıa Lactea, E-38200 La Laguna, Tenerife, Canary

Islands, Spain;

idelgado@iac.es, cmt@iac.es

Instituto Nacional de Astrofısica, Optica y Electronica, AP 51, 72000 Puebla, Mexico;

gtt@inaoep.mx

Special Astrophysical Observatory, 369167 Nizhnij Arkhyz, Russia;

moisav@sao.ru

Astrophysikalisches Institut Postdam, An der Sternwarte 16, D-14482 Potsdam, Germany;

luzma@aip.de

ABSTRACT

Here we present the analysis of 3D spectroscopic data of three Blue Compact

Galaxies (Mrk 324, Mrk 370, and III Zw 102). Each of the more than 22500

spectra obtained for each galaxy has been fitted by a single gaussian from which

we have inferred the velocity dispersion (σ), the peak intensity (Ipeak), and the

central wavelength (λc). The analysis shows that the σ vs Ipeak diagrams look

remarkably similar to those obtained for giant extragalactic H II regions. They

all present a supersonic narrow horizontal band that extends across all the range

of intensities and that result from the massive nuclear star-forming regions of

every galaxy. The σ vs Ipeak diagrams present also several inclined bands of

lower intensity and an even larger σ, arising from the large galactic volumes that

surround the main central emitting knots. Here we also show that the σ vs λc

and λc vs Ipeak diagrams, are powerful tools able to unveil the presence of high

and low mass stellar clusters, and thus allow for the possibility of inferring the

star formation activity of distant galaxies, even if these are not spatially resolved.

Subject headings: galaxies: spectroscopy — galaxies: individual(Mrk 370, Mrk 324,

III Zw 102) –galaxies: dwarfs — galaxies: starbursts

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1. Introduction

High resolution panoramic spectroscopy with good spatial and spectral resolution is

known to be a powerful tool for studying the kinematics of ionized nebulae as it leads

to a simultaneous mapping, at seeing limited resolution, of a particular emission line over

the whole nebula. This however can easily lead to several tens of thousands of spectra,

making it difficult to issue a detailed and/or a global interpretation of the data. An analysis

procedure that has proven to be simple and powerful results from fitting a single gaussian

to each of the resultant emission line profiles (see Munoz-Tunon 1994; Munoz-Tunon et al.

1995). A single gaussian regardless of the actual degree of asymmetry or splitting in the

line profiles. The fit is to conserve the flux of the line profile, and thus lower intensity but

broader lines would result from the most asymmetric or largely splitted line profiles. From

the resultant fits one can derive the velocity dispersion (σ), the peak intensity (Ipeak) of the

fitted lines as well as their central wavelength (λc). Such a method when applied to giant

extragalactic H II region (GHIIR) data, leads to two distinct regions in the σ vs Ipeak diagram

(see Munoz-Tunon et al. 1996): A supersonic (σ > cH II), relatively narrow horizontal band

with all possible peak intensity values, and a second region populated by lower intensity

points presenting even larger supersonic σ values, that crowd along multiple inclined bands.

For the case of GHIIRs it has been shown (see Munoz-Tunon 1994; Munoz-Tunon et al.

1996; Sabalisck et al. 1995; Fuentes-Masip et al. 2000; Telles et al. 2001, the last reference

for the case of H II Galaxies data) that the horizontal band is conformed by data with

truly gaussian profiles arising mainly from the brightest portions of the nebula, from the

small regions that enclose groups or clusters of stars. The inclined lower intensity and

highly supersonic bands on the other hand, emanate from multiple photoionized shells that

surround the star-forming centers and are likely to result from the stellar mechanical energy

impact into the ISM, and thus from single gaussian fits to highly asymmetric or strongly

splitted lines. The analysis of the σ vs Ipeak diagram for GHIIRs in nearby galaxies (closer

than 1 Mpc) was then proposed as an excellent tool to determine their degree of evolution on

kinematic bases (Munoz-Tunon et al. 1996). Here we extend the analysis to Blue Compact

Galaxies (BCGs) at even larger distances and show that they experience a similar dynamical

evolution (ie. their σ vs Ipeak diagrams look very much like those of GHIIRs). We further

extend our analysis by looking also at the σ vs λc and λc vs Ipeak diagrams, and show them

as ideal tools to distinctly unveil the presence of high and low mass stellar clusters.

Here section 2 provides a short description of the observations. Section 3 contains a

detailed analysis of the data by means of the diagnostic diagrams here proposed and section

4 gives a summary and a discussion of our findings.

– 3 –

2. The observations

We use the 6m Big Telescope Alta-azimuthal (BTA) of the Special Astrophysical Ob-

servatory (SAO) in Nizhnij Arkhyz (Russia), equipped with the multi-mode focal reducer

SCORPIO1 in the scanning Interferometer Fabry-Perot (IFP) observational mode (see Afanasiev & Moiseev

2005), for the observations of three BCGs: Mrk 370, III Zw 102, and Mrk 324. SCORPIO

is provided with a EEV 42-40 CCD array of 2048 × 2048 pixels with an instrumental scale

of 0.18 ′′ pixel−1. A set of interference filters centered at the Hα line, covering an interval of

systemic velocities that range from −200 to 10000 km s−1, is used at the IFP observational

mode. The IFP offers two configuration depending on the interference order, in our case at

the Hα line, the IFP260 (at the interference order 235) and the IFP500 (at the interference

order 501). Our observation runs were performed using the IFP500 mode, that offers a better

spectral resolution in the Ha emission line.

The output from the IFP results on a 3D data cube with x and y being the spatial

plane and z the wavelength sampling or ethalon step, that in the case of IFP500 mode, it

translates into 32-40 channels. The original data cube dimensions were (522,522,36) although

for our analysis we reduced the size, matching the objects size, to (150,150,36). The Free

Spectral Range (FSR) was 13 A, enough to sample the Hα line, that was scanned with a

spectral sampling of 0.7 A ≈ 32 km s−1. A binning of 4×4 pixels was applied in the spatial

directions in order to reduce the time exposure and improve the signal to noise of the final

data cube, resulting in a final spatial scale of 0.7 ′′ pixel−1. The instrumental width taken

from a fitting of the calibration lamp data cube was σinst = 20 ± 3 km s−1. Table 1 lists

a log of the observations together with some data about the galaxies: Column 1 gives the

name of the object; columns 2 and 3 show the coordinates (from NED2); columns 4 shows

the linear scale for each galaxy; column 5 lists the total time exposure of the observations;

column 6 gives the seeing conditions; column 7 shows the systemic velocity of each galaxy

and column 8 gives the distance in Mpc. Each of our SCORPIO trimmed data cubes contains

a total of 22500 spectra from an area of ∼3 arcmin2. The bulk of the data thus requires of

automatic techniques of analysis to extract the full power of 3D spectroscopy. For each of the

three galaxies, their Hα emission lines in every pixel were fitted by single gaussians, to then

obtain their Ipeak, σ, and λc, as described in Munoz-Tunon et al. (1995, 1996). The velocity

dispersion is given in km s−1 and is corrected for the instrumental and thermal broadening

(σ2 = σ2

obs − σ2

inst − σ2

th). We then used MoisSoft, the software package designed for the

1http://www.sao.ru/hq/lsfvo/devices/scorpio/scorpio.html

2NASA/IPAC Extragalactic Database is operated by the Jet Propulsion Laboratory, California Institute

of Technology, under contract with the National Aeronautics and Space Administration(NASA).

– 4 –

manipulation of SCORPIO-IFP spectral line data cubes. For a detailed explanation about

the data reduction procedure, see Moiseev (2002).

3. Three Dimensional Spectroscopy of BCDs

3.1. Mrk 324

Mrk 324 is a galaxy classified as a Blue Compact Dwarf (BCD, see Thuan & Martin

1981) and is included as a Nucleated BCD in the morphological classification of Cairos

et al. (2001), as it is basically powered by a luminous central knot. The star formation

history of the galaxy fits well with an instantaneous star formation law with a Salpeter IMF

(α = 2.35) and a range of masses between 1≤ M/M⊙ ≤100, in which a central knot of

4.4 Myr and 1.4×105 M⊙ in stars dominates 95% of the emission flux of the galaxy (see

Martınez-Delgado et al. 2006).

Figure 1 (upper row of panels) shows the results from the single gaussian fit to the full

Hα SCORPIO data set in the σ vs Ipeak, σ vs λc, and λc vs Ipeak diagrams for Mrk 324. The

last frame, upper row, shows the Hα image of the nucleated galaxy (see Cairos et al. 2001)

obtained at the NOT 2.52m telescope of the Roque de Los Muchachos Observatory (ORM)

in La Palma (Spain). The resemblance of the σ vs Ipeak diagram with those of GHIIRs is

remarkable. It presents a horizontal band that limits the values of σ to supersonic values (σ

≥ 20 km s−1) and a bunch of low intensity points at even higher σ values, that delineate a

triangular structure above the horizontal band. If one selects from the σ vs Ipeak diagram

the highest intensity data points, those belonging to the horizontal band (see second row of

panels in Figure 1), these in the σ vs λc diagram appear clumped at a given λc (∼ 6598.2

A) what implies that they all arise from a very similar location in the galaxy, that they all

belong in principle to a single entity. Note however, that this is not exactly coincident with

the rest wavelength of the galaxy (marked in the λc plots with a red line, see Figure 1).

The selected points in the λc vs Ipeak diagram defined also a pointed structure towards high

intensity values. These points in the emission-line peak intensity map (last frame) display

their location in the galaxy, which indeed coincides with the major burst of star formation

in Mrk 324. A major burst with an estimated mass in stars ∼ 4 × 105 M⊙ and an age of

about 4.4 Myr (see Martınez-Delgado 2005; Martınez-Delgado et al. 2006) that causes an H

II region with a radius of ∼ 250 pc. On the other hand, the data belonging to the inclined

bands with a higher velocity dispersion and a lower intensity in the σ vs Ipeak diagram (see

third row of panels in Figure 1) appear well scattered in λc and arise from a large-scale (600

pc in thickness) expanding rim that surrounds the central emitting knot, as shown in the last

panel of the third row. The inserts in the last column of Figure 1 display the Hα line and its

– 5 –

single gaussian fit at various locations in the galaxy. As in GHIIRs, the data corresponding

to the horizontal band in the σ vs Ipeak diagram leads to the highest intensity true gaussian

profiles, while the profiles fitted to lower intensity and larger σ data points, arising from the

outer expanding rim, are fits to asymmetric and/or double peak line profiles. Figure 1 shows

the quality of typical line profiles from each of the regions, displaying their intensity, central

wavelength, and σ values.

3.2. Mrk 370

This BCD galaxy belongs to the Chained morphological type (see Cairos et al. 2001),

in which the star formation takes place along a privileged direction. It follows the same

star formation law as Mrk 324, with 25 young and massive exciting clusters hosted over

an underlying stellar component with ages larger than 5 Gyr, (see Cairos et al. 2002). The

clusters have an average age of 6.6 Myr with a dispersion of 0.9 Myr, suggesting a coeval

and global star formation event. For the ones located in the inner nuclear region, the stellar

mass content reaches up to several 105 M⊙, (see Martınez-Delgado et al. 2006).

Figure 2 displays similar diagnostic diagrams for Mrk 370. The last frame in the upper

row of panels shows the Hα image of the chained galaxy (see Cairos et al. 2001) obtained at

the CAHA 2.2m telescope of the Centro Astronomico Hispano Aleman (CAHA), from Calar

Alto Observatory (Spain). The ionized gas in Mrk 370 (see the Hα image in Figure 2) presents

much more structure than Mrk 324. However, its σ vs Ipeak diagram looks almost identical

to that shown in Figure 1 for Mrk 324. The only exception is perhaps the low intensity data

points with values of σ below the supersonic lower limit imposed by the horizontal band (≤

21 km s−1, see first panel in Figure 2). The structure of the photoionized gas in Mrk 370

begins to be disentangled when one selects the data from the horizontal band in the σ vs

Ipeak diagram (see Figure 2, second row of panels). Such a data set appears clumped at three

different λc values in the σ vs λc diagram. The brightest one sits at the rest wavelength

of the galaxy (6580.1A). There is a second one at ∼6579.4A and a third one between these

two at ∼6579.8A. Two of them are much more apparent in the λc vs Ipeak diagram where

they clearly end up as pointed structures with different intensity (factors of 2) and different

central wavelengths. The emission-line peak intensity map tracing the selected points (last

frame in the second row) shows two major bursts of stellar formation and two adjacent much

less intense, associated to the massive central stellar clusters with masses that range between

(8−50)×104 M⊙ (see Martınez-Delgado 2005; Martınez-Delgado et al. 2006), also resolved

by Cairos et al. (2002) using the INTEGRAL spectrograph with a single gaussian fit to the

emission lines. All of these, although near the center of the galaxy, are kinematically resolved

– 6 –

as well detached structures. This multiplicity of structures would have been missed if one

had only use the σ vs Ipeak diagram as a diagnostic for this galaxy (see first panel in Figure 2),

as the brightest points present almost the same supersonic gaussian profiles. These massive

regions also match the area of the galaxy that shows the highest ionization values (see the

Hα emission-line and the [OIII]/Hβ maps in Cairos et al. 2002).

The third row of panels in Figure 2 displays the data from the inclined bands with low

intensity and large σ values in the σ vs Ipeak diagram. This data set, as the corresponding

one in Mrk 324, presents a large range of values of λc, around the systemic velocity of the

galaxy. The spread of the data is also noticeable in the λc vs Ipeak plane. The bulk of the

data arises from a large galactic volume shown in the emission-line peak intensity map as an

expanding rim of gas around the main centers of star formation all over the galaxy. This is

most intense around the nuclear starburst zone and although less intense, it is still noticeable

around smaller bursts of stellar formation some 2 kpc away from the nuclear region.

The final row of panels show the low intensity and low velocity dispersion data from the

σ vs Ipeak diagram (see Figure 2), which appears as vertical well detached low σ structures

in the σ vs λc plane. These structures, given their low values of σ, detach well from the bulk

of the data, most of which presents supersonic values, and due to their largely different λc

values they also appear as well detached entities along the λ scale. Note however that given

their low intensity values, they are much less apparent in the λc vs Ipeak diagram. These

data points correspond in the emission-line peak intensity map (last panel in the 4th row

of Figure 2) to multiple knots of emitting gas, or H II regions excited by low mass stellar

groups (with masses ≤ 104 M⊙, see Martınez-Delgado 2005; Martınez-Delgado et al. 2006)

at large distances from the centre of the galaxy. The line profiles arising from these regions

are also gaussian profiles although with a very low intensity when compared to those arising

from the central starburst regions (see inserts in the last frame of Figure 2).

3.3. III Zw 102

This galaxy is believed to be the result of an interaction event (see Vorontsov-Velyaminov

1959; Vorontsov-Vel’Yaminov 1977) and has been considered by some authors to belongs to

the polar-ring galaxy type (Whitmore et al. 1990). It is morphologycally considered as an

Extended Blue Compact Galaxy (Cairos et al. 2001), in which 65 star-forming regions were

identified spreaded over the whole main body of the galaxy, including the arms. The age of

the knots and their low age dispersion (6.1 ± 0.6 Myr) suggest a coeval starburst event (see

Martınez-Delgado et al. 2006).

– 7 –

Figure 3 displays the results for III Zw 102. The last frame in the upper row of panels,

shows the Hα image of the extended galaxy (see Cairos et al. 2001) obtained at the NOT

2.52m telescope of the Roque de Los Muchachos Observatory (ORM) in La Palma (Spain).

The data for III Zw 102 confirms the power of all of the diagnostic diagrams here used.

The galaxy has a plethora of small H II regions spread along two arms as well as several

massive centers of stellar formation in the densest nuclear region with masses between ∼

105 − 106 M⊙, (see Martınez-Delgado 2005; Martınez-Delgado et al. 2006). All of these, as

well as the large galactic volumes undergoing a supersonic expansion leave their signature

in the diagnostic diagrams. In this way, the horizontal band with supersonic σ values at all

possible intensities noticeable in the σ vs Ipeak diagram (see Figure 3, 2nd row of panels) is

spread over a large range of λc values in the σ vs λc diagram and into at least four pointed

structures (at λc = 6596.7A, 6597.25A, 6598A, and 6600A) of different intensities in the λc

vs Ipeak diagram. All of these in the emission-line peak intesity map are well resolved as

giant structures within the galactic nuclear region. On the other hand, the larger σ points

at all peak intensities in the σ vs Ipeak diagram arise from gas expanding around the nuclear

zone (see third row of panels in Figure 3). Among this data set is the inclined structure

between Ipeak=1100-1400 which is produced by gas between the four major centers of stellar

formation in the nuclear region. The broad line structure appears at the center of the galaxy

with a λc very similar to the systemic velocity of III Zw 102.

Finally, the lowest σ and lowest intensity data points in the σ vs Ipeak diagram (last row

of panels in Figure 3) appear, as in the case of Mrk370, as a set of well detached vertical

stalactites in the σ vs λc diagram, hanging from the bulk of the data at very distinct λc values.

The latter as shown in the last panel are produced by the numerous small H II regions located

along the galactic arms. As shown by the inserts in the last column of panels, the quality of

the gaussian fits is totally different in the three regions. The nuclear zone shows supersonic

perfect gaussians while the surrounding gas presents much broader and asymmetric lines.

Single gaussians with small σ values fit well the data from small centers of star formation.

4. Summary

Tridimensional spectroscopy with good spatial and spectral resolution, sampling a par-

ticular emission line over the whole area covered by an emitting nebula, is known to be the

most suitable observational technique for analyzing the global kinematics of GHIIRs. In

particular if a single gaussian fit is carried out over the emission lines in every pixel and from

those, one infers the velocity dispersion, the central wavelength, and the peak intensity of

the lines. The resultant σ vs Ipeak diagram (Munoz-Tunon et al. 1996) has been shown to

– 8 –

be an excellent diagnostic diagram to separate the main broadening mechanisms affecting

the emission lines, e.g., those that lead to shells and loops generated by the violent action

from massive stars (see Dyson 1979, Roy et al. 1986) which finally lead to cloud dispersal,

and the one(s) affecting the regions of massive star formation (either gravity; see Terlevich

& Melnick 1981, Tenorio-Tagle et al. 1993, or turbulence; see Chu & Kennicutt 1994). The

sequences shown by the various GHIIRs so far analyzed, led the authors also to propose the

σ-Ipeak plot as a tool able to trace the evolutionary status of a GHIIR, from its formation to

the total dispersal of the ionized gas.

Here we have confirmed that the data from the inclined supersonic bands in the σ vs

Ipeak diagrams are caused by the mechanical energy deposited by massive stellar sources.

These, depending on the age of the stellar clusters and on the density of the surrounding

gas may affect small or large galactic volumes. However in all cases, the interaction leads to

very asymmetric line profiles, evident in the σ vs Ipeak diagram for their highly supersonic σ

values.

Here we have extended the analysis to Blue Compact Galaxies. We have selected sources

with a single nuclear starburst (as Mrk 324) as well as galaxies with multiple stellar bursts

both within their nuclei as well as at large galactocentric distances. In all cases the σ vs Ipeak

diagram resembles those from GHIIRs in which the data define a supersonic σ (larger than

cH II ≈ 10 km s−1) horizontal band with all possible intensity values. Note that the value of

the limiting σ is different in every case. For III Zw 102 the horizontal band peaks at ∼ 33

km s−1, while for Mrk 324 and Mrk 370 it occurs at 24 and 25 km s−1, respectively.

The σ horizontal band, for the case of multiple massive nuclear bursts of stellar forma-

tion, has been shown to split into different bands in the λc vs Ipeak diagram. In this new

diagram, the largest nuclear regions of massive star formation become evident due to the

good spectral resolution. And thus even with a poor spatial resolution, or when dealing with

further away sources, the sampling of the velocity field, with our 3D spectrographs, would

reveal the exciting sources. Similarly, the σ vs λc new diagram picks up the small bursts of

stellar formation by tracing their lower intensity and slower expansion of their immediate

surroundings.

The stalactites detected in the σ vs λc diagram in the case of III Zw 102 and Mrk 370

correspond to the ionized knots located in the outskirts of the galaxies and their spread in

σ result from the H II regions expansion into a low density medium (see Franco et al. 1990).

On the whole, the new diagnostic diagrams here presented provide the possibility of

inferring from 3D spectroscopy, the magnitude of the star formation activity of distant

galaxies, even if these are not spatially resolved.

– 9 –

IMD acknowledges the FPI grant (FP-2001-2506) of the Spanish Government through

the collaboration of the project AYA2004-08260-C03-01 (ESTALLIDOS,

http://www.iac.es/project/GEFE/estallidos). AVM acknowledges the the Russian Founda-

tion for Basic Research (project 05-02-16454). This work is partly based on observations

carried out at the 6m telescope of the Special Astrophysical Observatory of the Russian

Academy of Sciences, operated under the financial support of the Science Department of

Russia (registration number 01-43), and it has been partly supported by the ESTALLIDOS

Project (AYA2004-08260-C03-01) and the grant AYA 2004-02703 from the Spanish Ministe-

rio de Educacion y Ciencia.

– 10 –

REFERENCES

Afanasiev, V. L., & Moiseev, A. V. 2005, Astronomy Letters, 31, 194

Cairos, L. M., Caon, N., Vılchez, J. M., Gonzalez-Perez, J. N., & Munoz-Tunon, C. 2001,

ApJS, 136, 2

Cairos, L. M., Caon, N., Garcıa-Lorenzo, B., Vılchez, J. M., & Munoz-Tunon, C. 2002, ApJ,

577, 164

Chu, Y.-H., & Kennicutt, R. C. 1994, ApJ, 425, 720

Dyson, J. E. 1979, A&A, 73, 132

Franco, J., Tenorio-Tagle, G., & Bodenheimer, P. 1990, ApJ, 349, 126

Fuentes-Masip, O., Munoz-Tunon, C., Castaneda, H. O., & Tenorio-Tagle, G. 2000, AJ, 120,

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Martınez-Delgado, I., 2005, DEA: Catalogues and Parameters of Starburst Knots in a

Sample of Blue Compact Dwarf Galaxies. Spain: University of La Laguna/Instituto

de Astrofııca de Canarias.

Martınez-Delgado, I., Munoz-Tunon, C.,, Cairos, L. M., Tenorio-Tagle, G. 2006, submitted

to AJ.

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Munoz-Tunon, C., 1994, Violent Star Formation: From 30 Doradus to QSOs. In: Tenorio-

Tagle G. (eds.). Cambridge University Press, p.25.

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Munoz-Tunon, C., Tenorio-Tagle, G., Castaneda, H. O., & Terlevich, R. 1996, AJ, 112, 1636

Roy, J.-R., Arsenault, R., & Joncas, G. 1986, ApJ, 300, 624

Sabalisck, N. S. P., Tenorio-Tagle, G., Castaneda, H. O., & Munoz-Tunon, C. 1995, ApJ,

444, 200

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Terlevich, R., & Melnick, J. 1981, MNRAS, 195, 839

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Thuan, T. X., & Martin, G. E. 1981, ApJ, 247, 823

Vorontsov-Velyaminov, B. A. 1959, VV, 0

Vorontsov-Vel’Yaminov, B. A. 1977, A&AS, 28, 1

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This preprint was prepared with the AAS LATEX macros v5.2.

–12

–

σ=46.0 km/s

σ=33.9 km/s

σ=23.9 km/s

σ=24.4 km/s

∆ x(")

∆y(

")

v(km/s)

Fig. 1.— The figure shows in the first row of panels the velocity dispersion σ vs peak intensity (the σ was corrected for the instrumental and

thermal broadening), for all the gaussian fits to the individual spectra of Mrk 324. The second and third panels display the corresponding σ

vs central lambda (λc, indicating also the velocity range in km s−1) and λc vs peak intensity, respectively. The solid line in these two panels

indicates the rest velocity of the galaxy. The last panel shows the Hα image of the galaxy and indicates its scale in kpc. The second and

following rows of panels highlight in colour the various sets of data points selected in the σ vs peak intensity diagram and their location in

the σ vs λc and λc vs peak intensity planes. The last panels in every row, with a peak intensity scale, display the locations in the galaxy

that produce the selected data points. Inserts in these panels correspond to typical gaussian fits (solid red lines) to the data arising from

different regions (axis correspond to intensity, in counts, vs the wavelength in A). The fitted σ values are indicated in every frame.

–13

–

Fig. 2.— Mrk 370. The same as Figure 1 for Mrk 370.

–14

–

Fig. 3.— III Zw 102. The same as Figure 1 for III Zw 102.

– 15 –

Table 1. Log of the Observations

Galaxy RA(2000) DEC(2000) Linear Scale(pc/′′) t(s) PSF(′′) VHI(km s−1) D(Mpc)

(1) (2) (3) (4) (5) (6) (7) (8)

Mrk370 02h40m29.s0 +19◦17′50′′ 52 4680 1.7 790† 10.85

IIIZw102 23h20m30.s1 +17◦13′32′′ 110 6480 1.8 1626† 22.71

Mrk324 23h26m32.s8 +18◦15′59′′ 108 4320 1.6 1600† 22.43

†Systemic velocity, from H I observations, corrected to the Local Group velocity centroid taken

from Thuan & Martin (1981).